It is possible to chop between two or three bolometers on the array, the main benefit being more time
spent on-source during the observation. The reduction of these data is very similar to the single
bolometer method shown in the preceeding section. The only recognizable difference is
that scucat will produce a concatenated output file for each bolometer. For example, if
data were taken simultaneously with the long-wavelength array pixels h7 and h9 and
the specified output file is
source1 then files
The most robust method of reducing these data is to observe a planet, such as Mars, in exactly the same way and then to calibrate each bolometer separately into flux units. The coadded result and its statistical uncertainty can then be calculated with standard formulae.